Mirror Matter: Astrophysical implications Zurab Berezhiani Summary Mirror Matter: Astrophysical implications Introduction: Dark Matter from a Parallel World Chapter I: Neutrino - mirror neutrino mixings Zurab Berezhiani Chapter II: neutron { mirror University of L'Aquila and LNGS neutron mixing Chapter IV: n − n0 and Neutron Stars Quarks-2021 , 22-24 June 2021 Contents Mirror Matter: Astrophysical implications Zurab Berezhiani Summary Introduction: Dark Matter from 1 Introduction: Dark Matter from a Parallel World a Parallel World Chapter I: Neutrino - mirror neutrino mixings 2 Chapter I: Neutrino - mirror neutrino mixings Chapter II: neutron { mirror neutron mixing Chapter IV: n − n0 and 3 Chapter II: neutron { mirror neutron mixing Neutron Stars 4 Chapter IV: n n0 and Neutron Stars − Mirror Matter: Astrophysical implications Zurab Berezhiani Summary Introduction: Dark Matter from a Parallel World Introduction Chapter I: Neutrino - mirror neutrino mixings Chapter II: neutron { mirror neutron mixing Chapter IV: n − n0 and Everything can be explained by the Standard Model ! Neutron Stars ... but there should be more than one Standard Models Bright & Dark Sides of our Universe Mirror Matter: Ω 0 05 observable matter: electron, proton, neutron ! Astrophysical B : implications ' ΩD 0:25 dark matter: WIMP? axion? sterile ν? ... Zurab Berezhiani ' ΩΛ 0:70 dark energy: Λ-term? Quintessence? .... Summary ' 3 Introduction: ΩR < 10− relativistic fraction: relic photons and neutrinos Dark Matter from a Parallel World Matter { dark energy coincidence: Ω Ω 0 45, (Ω = Ω + Ω ) Chapter I: M = Λ : M D B Neutrino - mirror 3 ' ρΛ Const., ρM a− ; why ρM /ρΛ 1 { just Today? neutrino mixings ∼ ∼ ∼ Chapter II: Antrophic explanation: if not Today, then Yesterday or Tomorrow. neutron { mirror neutron mixing Baryon and dark matter Fine Tuning: ΩB =ΩD 0:2 Chapter IV: 0 3 3 ' n − n and ρB a− , ρD a− : why ρB /ρD 1 - Yesterday Today & Tomorrow? Neutron Stars ∼ ∼ ∼ Baryogenesis requires BSM Physics: (GUT-B, Lepto-B, AD-B, EW-B ...) Dark matter requires BSM Physics: (Wimp, Wimpzilla, sterile ν, axion, ...) Different physics for B-genesis and DM? Not very appealing: looks as Fine Tuning Dark Matter from a Parallel World Mirror Matter: Astrophysical implications Our observable particles: (Best of the possible Worlds ....) Zurab Berezhiani G = SU(3) SU(2) U(1) ( + SUSY ? + GUT ? ... ) × × Summary electron, nucleons (quarks), neutrinos, gluons, Higgs Introduction: QED photon/long range, QCD gluons/confining, Weak W ; Z/short range Dark Matter from a Parallel World ... matter vs. antimatter (CP + B/B-L violation ... ) Chapter I: ... existence of nuclei, atoms, molecules .... life.... Homo Sapiens ! Neutrino - mirror neutrino mixings Dark matter: a parallel sector ? (Best of the possible Dark Worlds ...) Chapter II: neutron { mirror G 0 = SU(3)0 SU(2)0 U(1)0 ? ( + SUSY ? GUT 0? Seesaw ?) neutron mixing × × ... dark matter (CP + B0/B0-L0 violation ... ) ? Chapter IV: n − n0 and ... existence of dark nuclei, atoms, molecules ... life ... Homo Aliens ? Neutron Stars Call it Yin-Yang (in chinise, dark-bright) duality describes a philosophy how opposite forces are ac- tually complementary, interconnected and interde- pendent in the natural world, and how they give rise to each other as they interrelate to one another. E8 E 0 × 8 SU(3) SU(2) U(1) + SU(3)0 SU(2)0 U(1)0 × × × × Mirror Matter: G G 0 Astrophysical × implications Regular world Mirror world Zurab Berezhiani Summary Introduction: Dark Matter from a Parallel World Chapter I: Neutrino - mirror neutrino mixings Chapter II: neutron { mirror neutron mixing Two identical gauge factors, e.g. SU(5) SU(5)0, with identical field • × Chapter IV: contents and Lagrangians: = + 0 + n − n0 and tot mix Neutron Stars L L L L Mirror sector ( 0) is dark { or perhaps grey?( mix portals ) • L L ! MM is similar to standard matter, (asymmetric/dissipative/atomic) • but realized in somewhat different cosmological conditions (T 0=T 1) LR Exact parity G G 0 (Z2 or Z ): no new parameters in 0 • ! 2 L Cross-interactions between O & M particles • mix : new operators { new parameters! limited only by experiment! L Visible vs. Dark matter: ΩD=ΩB 1 ? ∼ Visible matter from Baryogenesis Mirror Matter: Astrophysical B (B L) & CP violation, Out-of-Equilibrium implications − 9 ρB = nB mB , mB 1 GeV, η = nB =n 10− Zurab Berezhiani ' γ ∼ is model dependent on several factors: Summary η Introduction: coupling constants and CP-phases, particle de- Dark Matter from a Parallel World grees of freedom, mass scales and out-of-equilibrium Chapter I: conditions, etc. Sakharov 1967 Neutrino - mirror neutrino mixings • Chapter II: Dark matter: ρD = nX mX , but mX = ? , nX = ? neutron { mirror neutron mixing nX is model dependent: DM particle mass and interaction strength Chapter IV: (production and annihilation cross sections), freezing conditions, etc. n − n0 and Neutron Stars 5 4 Axion ma 10− eV na 10 nγ - CDM ∼ 1 ∼ Neutrinos mν 10− eV nν nγ - HDM ( ) ∼ ∼ 3 × Sterile ν0 m 0 10 keV n 0 10− n - WDM ν ∼ ν ∼ ν Mirror baryons mB0 1 GeV nB0 nB - ??? ' ∼ 3 WIMP mX 1 TeV nX 10− nB - CDM ∼ 14 ∼ 14 WimpZilla mX 10 GeV nX 10− nB - CDM ∼ ∼ SU(3) SU(2) U(1) vs. SU(3)0 SU(2)0 U(1)0 × × × × Two possible parities: with and without chirality change Fermions and anti-fermions : Mirror Matter: Astrophysical implications uL νL qL = ; `L = ; uR ; dR ; eR Zurab Berezhiani dL eL B=1/3 L=1 B=1/3 L=1 Summary CP l Introduction: u¯R ¯ ν¯R ¯ Dark Matter from q¯R = ; `R = ;u ¯L; dL; e¯L d¯R e¯R a Parallel World Chapter I: B={1/3 L={1 B={1/3 L={1 Neutrino - mirror neutrino mixings Twin Fermions/anti-fermions : Chapter II: neutron { mirror neutron mixing uL0 νL0 qL0 = ; `L0 = ; uR0 ; dR0 ; eR0 Chapter IV: dL0 eL0 n − n0 and Neutron Stars B0={1/3 L0={1 B0={1/3 L0={1 CP l u¯R0 ¯ ν¯R0 ¯ q¯R0 = ; `R0 = ;u ¯L0 ; dL0 ; e¯L0 d¯0 e¯0 R R B0=1/3 L0=1 B0=1/3 L0=1 ¯ ¯ Yuk = FLY FLφ + h.c. 0 = F 0Y 0F 0φ0 + h.c. L LYuk L L Z2: L(R) L0(R0): Yu0;d;e = Yu;d;e B+B0 (B+B0) LR $ ! − LR Z : L(R) R0(L0): Y 0 = Y ∗ B+B0 B+B0 Z = Z2 CP 2 $ u;d;e u;d;e ! 2 × { Sign of baryon asymmetry (BA)? Mirror Matter: Astrophysical Ordinary BA is positive: = sign(nb nb¯) = 1 implications { as produced by (unknown)B baryogenesis− a la Sakharov! Zurab Berezhiani Sign of mirror BA, 0 = sign(nb0 nb¯0 ), is a priori unknown! Summary B − Introduction: Imagine a baryogenesis mechanism separately acting in O and M sectors! Dark Matter from { without involving cross-interactions in mix a Parallel World L Chapter I: E.g. EW baryogenesis or leptogenesis N `φ and N0 `0φ0 Neutrino - mirror ! ! neutrino mixings Z2: Yu0;d;e = Yu;d;e i.e. 0 = 1 Chapter II: ! B − neutron { mirror { O and M sectors are CP-identical in same chiral basis! O=left, M=left neutron mixing LR Chapter IV: Z2 : Yu0;d;e = Yu∗;d;e i.e. 0 = 1 0 ! B n − n and { O sector in L-basis is identical to M sector in R-basis! O=left, M=right Neutron Stars In the absence of cross-interactions in mix we cannot measure sign of BA or chirality in weak interactions of M sectorL { so all remains academic ... But switching on cross-interactions, violating B and B0 { but conserving say B+B0 as e.g. neutron{mirror neutron (n n0) mixing: nn0 + h:c: LR − Z 0 = 1 n0 n M matter O matter 2 !B ! ! ! Z2 0 = 1 n0 n M (anti)matter O antimatter !B − ! ! ! { All you need is ... M world colder than ours ! For a long time M matter was not considered as a real candidate for DM: Mirror Matter: Astrophysical naively assuming that exactly identical microphysics of O & M worlds implications implies also their cosmologies are exactly identical : Zurab Berezhiani eff eff T 0 = T , g 0 = g ∆Nν = 6:15 vs. ∆Nν < 0:5 (BBN) Summary • ∗ ∗ ! Introduction: nB0 =nγ0 = nB =nγ (η0 = η) ΩB0 = ΩB vs. ΩB0 =ΩB 5 (DM) Dark Matter from • ! ' a Parallel World But all is OK if : Z.B., Dolgov, Mohapatra, 1995 (broken Z2) Chapter I: Neutrino - mirror Z.B., Comelli, Villante, 2000 (exact Z2) neutrino mixings Chapter II: neutron { mirror A. after inflation M world was born colder than O world, TR0 < TR neutron mixing B. any interactions between M and O particles are feeble and cannot bring Chapter IV: n − n0 and two sectors into equilibrium in later epochs Neutron Stars C. two systems evolve adiabatically (no entropy production): T 0=T const ' T 0=T < 0:5 from BBN, but cosmological limits T 0=T < 0:2 or so. 4 x = T 0=T 1= in O sector 75% H + 25% He ) 4 = in M world 25% H0 + 75% He0 ) For broken Z2, DM can be compact H' atoms or n0 with m 5 GeV or (sterile) mirror neutrinos m few keV Z.B., Dolgov, Mohapatra,' 1995 ∼ Brief Cosmology of Mirror World CMB & (linear) structure formation epoch Mirror Matter: • Astrophysical Since x = T 0=T 1, mirror photons decouple before M-R equality: implications 1 z 0 x − z 1100 (T =T 0) Zurab Berezhiani dec dec After' that (and' before M{reionization) M matter behaves as collisionless Summary CDM and T 0=T < 0:2 is consistent with Planck, BAO, Ly-α etc. Introduction: Dark Matter from Cosmic dawn: M world is colder (and helium dominated), the first M a Parallel World • star can be formed earlier and reionize M sector (z 0 20 or so vs zr 10).